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The Long-term Variation in the RV Tauri Star U Mon

Published online by Cambridge University Press:  12 April 2016

Karen R. Pollard  and
P. L. Cottrell
Karen R. Pollard
Affiliation:
Mt John University Observatory, Department of Physics & Astronomy, University of Canterbury, Christchurch, New Zealand
P. L. Cottrell
Affiliation:
Mt John University Observatory, Department of Physics & Astronomy, University of Canterbury, Christchurch, New Zealand

Extract

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The RV Tauri stars are semiregular pulsating variables located in the brightest part of the Cepheid II instability strip. They have a characteristic light curve of alternating deep and shallow minima. A subset of the RV Tauri stars (the RVb subclass) exhibit long-term (500 to 2600 day) light and radial velocity variations. Although it is well established that the short-term variations are due to pulsations, the long-term behaviour is not well understood.

BVRI photometry and high-resolution spectra of U Mon (the brightest member of the RVb subclass) were obtained at the Mt John University Observatory (MJUO) between 1990 Aug and 1994 May. The light and colour curves obtained clearly show the long-term variation in U Mon (Fig. 1(a) and (b)). The reddest colours occur slightly later than the long-term minimum in the light curve. The short-term light and colour variations are ‘damped’ at the long-term minimum.

Type
Part 2. Poster Papers
Information
International Astronomical Union Colloquium , Volume 155: Astrophysical Applications of Stellar Pulsation , 1995 , pp. 409 - 410
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

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